Contraction models for the evolution of Jupiter

Details Contraction models for the evolution of Jupiter Contraction models for the evolution of Jupiter

Oct 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976icar...29..165b&link_type=abstract

(IAU, NASA, and NSF, Jupiter Colloquium, 30th, Tucson, Ariz., May 18-23, 1975.) Icarus, vol. 29, Oct. 1976, p. 165-171.

Astronomy and Astrophysics

Astronomy

9

Contraction, Gravitational Collapse, Jupiter (Planet), Planetary Evolution, Astronomical Models, Energy Transfer, Luminosity, Planetary Nebulae

Scientific paper

The evolution of Jupiter is discussed under the hypothesis that the planet formed as a subcondensation in the solar nebula with a density just high enough that it would be gravitationally bound. Numerical calculations show that the evolution consists of two major phases: (1) a radiative protoplanetary contraction in quasi-hydrostatic equilibrium followed by hydrodynamic collapse and (2) a convective quasi-static contraction during which the planet approaches its present radius. The consistency between existing calculations of these two phases is discussed, and the basic assumptions used in such calculations are critically examined.

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